Antenna-coupled TES Arrays For The BICEP2∕Keck and SPIDER polarimeters

Orlando, A.; Aikin, R. W.; Amiri, M.; Bock, J. J.; Bonetti, J. A.; Brevik, J. A.; Burger, B.; Day, Peter; Filippini, J. P.; Golwala, S. R.; Halpern, M.; Hasselfield, Matthew; Hilton, G. C.; Irwin, K. D.; Jones, W. C.; Kenyon, M.; Kuo, Chao-Lin; Lange, A. E.; Leduc, H. G.; Mates, B.; Morford, T. A.; Nguyen, Hien; Ogburn, R. W.; Reintsema, C. D.; Runyan, M. C.; Sudiwala, R.; Trangsrud, A.; Turner, Anthony; Wilson, P.

doi:10.1063/1.3292380

Cited by 7 publications

(8 citation statements)

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“…However, measurements with a chopped load indicate that the dominant out-of-band response mechanism has a time constant of ∼ 10 ms, significantly faster than has been previously measured for the tile heating in similar instruments. 21 Additionally, Figure 7(a) has labels indicating the approximate distance from the edge of the cover. All three of the tested devices show a response that decreases with distance from the edge, a phenomenon poorly explained by tile heating where we expect the entire silicon substrate to be isothermal but well explained by an optical signal that experiences partial attenuation as it propagates in the lossy materials packed in front of the tile over the bolometer banks.…”

Section: Optical Characterizationmentioning

confidence: 99%

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Lithographed spectrometers for tomographic line mapping of the Epoch of Reionization

et al. 2014

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The Tomographic Ionized carbon Mapping Experiment (TIME) is a multi-phased experiment that will topographically map [CII] emission from the Epoch of Reionization. We are developing lithographed spectrometers that couple to TES bolometers in anticipation of the second generation instrument. Our design intentionally mirrors many features of the parallel SuperSpec project, inductively coupling power from a trunk-line microstrip onto half-wave resonators. The resonators couple to a rat-race hybrids that feeds TES bolometers. Our 25 channel prototype shows spectrally positioned lines roughly matching design with a receiver optical efficiency of 15-20%, a level that is dominated by loss in components outside the spectrometer. ASTROPHYSICAL MOTIVATIONThe Epoch of Reionization (EoR) is an era during which ultraviolet emission from the first generation of stars in the Universe ionized the intergalactic medium in a process which was completed by z ∼ 6 1 . 2 Because of the distance to and intrinsic low luminosity of EoR sources, this era remains poorly understood. The Lyman-α break renders measurements at λ 1 µm sensitive only to the end of reionization, making infrared and radio measurements of EoR emission attractive. 3 Several teams, such as PAPER, LOFAR, and MWA are attempting to use the hyperfine transition in neutral hydrogen at λ = 21 cm line as a tracer of structure during and prior to the EoR. In contrast to the Lyman-α line, the 21 cm transition has an extremely low scattering cross-section so avoids the short mean free path that renders the EoR opaque to optical and near-infrared photons. By generating maps at different redshifts, these experiments can trace neutral hydrogen's density and structure over time, producing a history of reionization. 4 In practical terms, these experiments engage in intensity mapping, a powerful technique in which the average emission over large regions is measured, and statistical techniques are used to infer bulk properties of the emission. 5 However, challenges abound: the signal is faint, and redshifts into the range ν =150-250MHz where interference from galactic and commercial radio sources are a significant foreground to the measurement. Cross-correlation of 21 cm maps with those of other atomic lines that originate during EoR effectively removes the foregrounds from either measurement, thereby improving the accuracy and power of both. 6 TIME will map ionized carbon [CII] as a complimentary means of tracing reionization history. The 158 µm [CII] line has significantly longer wavelength than can interact with neutral hydrogen so should be visible to large redshifts. Additionally, because it is a significant cooling mechanism in star formation and accounts for up to ∼ 1% of the bolometric power from star-forming galaxies, the 158 µm line should be bright in systems in which carbon is present. 7 Furthermore, 158 µm emission between z = 9 and z = 5 redshifts into the 200-300 GHz atmospheric window, permitting observations from ground-based instruments that can provide the necessary...

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Section: Optical Characterizationmentioning

confidence: 99%

“…21 The design bandwidth of our spectrometer channels is roughly 0.6GHz, 2% of the 150GHz TES polarimeters' bandwidth. With this greatly reduced loading through the microstrip circuits, direct stimulation is proportionately larger; in an optical design similar to BICEP2, the spectrometer channels would experience 30% direct stimulation.…”

Section: Pixel Prototypementioning

confidence: 99%

Lithographed spectrometers for tomographic line mapping of the Epoch of Reionization

et al. 2014

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“…Having achieved reproducible and uniform device parameters, 6 we decided to optimize target thermal conductivities, aiming to G c ∼ 20 pW/K for SPIDER and G c ∼ 80 pW/K for BICEP2/Keck (at T c ∼ 510 − 520 mK). Tests performed on few engineering detector arrays confirmed we can achieve the new targets and easily optimize performances with optical loading.…”

Section: Device Parameters and Arrays Uniformitymentioning

confidence: 99%

“…BICEP2/Keck and SPIDER focal planes employ planar arrays of dual-polarization antenna-coupled TES bolometers operating at frequencies between ∼ 90 GHz and 220 GHz . At the LTD13 conference we reported our early progress in characterizing engineering focal plane arrays 6 and SQUID multiplexed readout for BICEP2 and SPIDER and our progress in microfabrication. 7 Having achieved consistently high fabrication yield and reproducible and uniform device parameters, we have since then focused on characterizing and optimizing focal plane optical properties and sensitivity.…”

Section: Introductionmentioning

confidence: 99%

Antenna-coupled TES bolometer arrays for BICEP2/Keck and SPIDER

et al. 2010

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BICEP2/Keck and SPIDER are cosmic microwave background (CMB) polarimeters targeting the B-mode polarization induced by primordial gravitational waves from inflation. They will be using planar arrays of polarization sensitive antenna-coupled TES bolometers, operating at frequencies between 90 GHz and 220 GHz. At 150 GHz each array consists of 64 polarimeters and four of these arrays are assembled together to make a focal plane, for a total of 256 dual-polarization elements (512 TES sensors). The detector arrays are integrated with a time-domain SQUID multiplexer developed at NIST and read out using the multi-channel electronics (MCE) developed at the University of British Columbia. Following our progress in improving detector parameters uniformity across the arrays and fabrication yield, our main effort has focused on improving detector arrays optical and noise performances, in order to produce science grade focal planes achieving target sensitivities. We report on changes in detector design implemented to optimize such performances and following focal plane arrays characterization. BICEP2 has deployed a first 150 GHz science grade focal plane to the South Pole in December 2009.

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“…5,6 Bicep2 and the Keck Array use a new detector technology, the Caltech-JPL antenna-coupled TES arrays. 7,8 These detectors are read out using NIST SQUID amplifiers with the University of British Columbia MCE control and Measured far-field beam maps for a single Keck Array receiver (rx1). This image was made from data taken at the South Pole in February 2012 using a thermal source raised on a mast.…”

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confidence: 99%

BICEP2 and Keck array operational overview and status of observations

et al. 2012

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The Bicep2 and Keck Array experiments are designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 2-4 degrees (ℓ = 50-100). This is the region in which the B-mode signal, a signature prediction of cosmic inflation, is expected to peak. Bicep2 was deployed to the South Pole at the end of 2009 and is in the middle of its third year of observing with 500 polarization-sensitive detectors at 150 GHz. The Keck Array was deployed to the South Pole at the end of 2010, initially with three receivers-each similar to Bicep2. An additional two receivers have been added during the 2011-12 summer. We give an overview of the two experiments, report on substantial gains in the sensitivity of the two experiments after post-deployment optimization, and show preliminary maps of CMB polarization from Bicep2.

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Antenna-coupled TES Arrays For The BICEP2∕Keck and SPIDER polarimeters

Cited by 7 publications

References 1 publication

Lithographed spectrometers for tomographic line mapping of the Epoch of Reionization

Lithographed spectrometers for tomographic line mapping of the Epoch of Reionization

Antenna-coupled TES bolometer arrays for BICEP2/Keck and SPIDER

BICEP2 and Keck array operational overview and status of observations

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